Using Monte Carlo techniques, we simulate the birth and evolution of millisecond pulsars. We model the spatial distribution of millisecond pulsars by assuming that they start with a random kick velocity and then evolve through the Galactic potential. We explore both uniform and non- uniform spatial birth distributions within the Galactic plane. After evolution, the radio and gamma-ray fluxes are compared to minimum fluxes for 10 radio surveys and three gamma-ray detectors. An approximation to the birth line dependence on mass accretion rate during spin-up described in Lamb and Yu (2005) has been incorporated into the simulations. We set a random accretion rate between 10-4 and 1 times the Eddington limit, and calculate the birth period, period derivative, and magnetic field based on this accretion rate. Using these new birth characteristics and including several other changes to the program, we obtain good agreement with observed distributions of millisecond pulsars.

*This material is based upon work supported
by the National Science Foundation under NSF-REU Grant No. 0452206.

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